N-body simulations of the dynamical evolution of rotating star clusters in galactic tidal field

N-body simulations of initially rotating star clusters to investigate quantitatively the influence of internal rotation and effects of galactic gravitational field on dynamical evolution of globular clusters is presented. NBODY6, which calculates the force acting on each particle was used to take into account the time dependent external gravitational field. The initial models of clusters were the rotating King models with a specified dimensionless central potential and dimensionless angular velocity. Experimental observation showed that the rotating clusters with a mass function lose their own mass significantly faster than non-rotating ones, and the tidal tails of initially rotating cluster have the same properties with initially non-rotating clusters in direction and length. It was found that the sense of internal rotation of the outer part becomes opposite to that of initial one after several revolutions, while the inner part remembers the initial sense of rotation for a long time.